Magnetized massive stars as magnetar progenitors
... 1995). By magnetic flux conservation during the stellar evolution, Ferrario & Wickramasinghe (2005) argued that stellar magnetic fields (∼100 G) in their main-sequence phase can be enhanced up to the range of ∼106 –109 G on the surface of magnetic white dwarfs. This fossil-field scenario is supporte ...
... 1995). By magnetic flux conservation during the stellar evolution, Ferrario & Wickramasinghe (2005) argued that stellar magnetic fields (∼100 G) in their main-sequence phase can be enhanced up to the range of ∼106 –109 G on the surface of magnetic white dwarfs. This fossil-field scenario is supporte ...
Microscopic vortex velocity in the inner crust and outer core of
... The physical state of the inner crust with its neutron rich nuclei and dripped neutron superfluid interspersed with them is well established since the pioneering work of Negele & Vautherin (1973). The superfluid density inside a nucleus is found to be somewhat larger than the outside dripped superfl ...
... The physical state of the inner crust with its neutron rich nuclei and dripped neutron superfluid interspersed with them is well established since the pioneering work of Negele & Vautherin (1973). The superfluid density inside a nucleus is found to be somewhat larger than the outside dripped superfl ...
Latitudinal and radial gradients of galactic cosmic ray protons in the
... The main scientific goal of the joint ESA-NASA Ulysses deep-space mission was to make the first-ever measurements of the unexplored region of space above the solar poles. The GCR intensity measured along the Ulysses orbit results from a combination of temporal and spatial variations. Ulysses was lau ...
... The main scientific goal of the joint ESA-NASA Ulysses deep-space mission was to make the first-ever measurements of the unexplored region of space above the solar poles. The GCR intensity measured along the Ulysses orbit results from a combination of temporal and spatial variations. Ulysses was lau ...
The ionized gas in the central region of NGC 5253
... With the limited spectral range utilized in that work, we could only determine relative nitrogen abundances. The most natural explanation for the interpretation of the increase of [N ii]λ6584/[S ii]λλ6717,6731 was an enhancement in nitrogen abundance; an interpretation supported by previous observat ...
... With the limited spectral range utilized in that work, we could only determine relative nitrogen abundances. The most natural explanation for the interpretation of the increase of [N ii]λ6584/[S ii]λλ6717,6731 was an enhancement in nitrogen abundance; an interpretation supported by previous observat ...
Dark Matter: A Brief Review
... dark matter, one typically must introduce some non-standard cosmology [20]. Heavy gravitinos are, in my opinion, more interesting. If the next-lightest supersymmetric particle (NLSP) is only barely more massive than the gravitino, that particle species may be thermally produced and then decay at a l ...
... dark matter, one typically must introduce some non-standard cosmology [20]. Heavy gravitinos are, in my opinion, more interesting. If the next-lightest supersymmetric particle (NLSP) is only barely more massive than the gravitino, that particle species may be thermally produced and then decay at a l ...
Testing Warm Dark Matter Model with Dwarf Galaxies
... Is dark matter from decays just a oneparameter family of models? Louie Strigari, UC Irvine ...
... Is dark matter from decays just a oneparameter family of models? Louie Strigari, UC Irvine ...
POLYTROPES - Princeton
... of a planet like Earth. The case n = 5 is also special, as the radius of this ”star” is infinite. It is possible to show that all polytropes with n > 5 have infinite radii. This means that only solutions with n < 5 have a surface. The two cases most interesting for real stars have n = 1.5 and n = 3, ...
... of a planet like Earth. The case n = 5 is also special, as the radius of this ”star” is infinite. It is possible to show that all polytropes with n > 5 have infinite radii. This means that only solutions with n < 5 have a surface. The two cases most interesting for real stars have n = 1.5 and n = 3, ...
Phase-resolved high-resolution spectrophotometry of the eclipsing
... field, which leads the matter along magnetic field lines to the polar regions of the white dwarf. Most of the gravitational energy is released there, although some dissipative energy loss is expected to occur all along the stream, in particular in the coupling region where the stream is forced to le ...
... field, which leads the matter along magnetic field lines to the polar regions of the white dwarf. Most of the gravitational energy is released there, although some dissipative energy loss is expected to occur all along the stream, in particular in the coupling region where the stream is forced to le ...
the inclination of the dwarf irregular galaxy
... galaxies with low inclinations, where traditional methods are less precise. We will focus on the dwarf irregular galaxy Holmberg II (Ho II) or DDO 50. From tiltedring models, Oh et al. (2011) derived a mean inclination angle of 49◦ . For this inclination, the asymptotic (flat) circular velocity Ho I ...
... galaxies with low inclinations, where traditional methods are less precise. We will focus on the dwarf irregular galaxy Holmberg II (Ho II) or DDO 50. From tiltedring models, Oh et al. (2011) derived a mean inclination angle of 49◦ . For this inclination, the asymptotic (flat) circular velocity Ho I ...
THREE Li-RICH K GIANTS - Indian Institute of Astrophysics
... the rapidly rotating K giant IRAS 175963952. Lines are weak to moderately strong (Wk 150 m8). Surface gravity ( log g) was obtained with the condition that the Fe i and Fe ii lines give the same abundance. The microturbulent velocity (t) was determined by requiring that the Fe i and Ni i lines g ...
... the rapidly rotating K giant IRAS 175963952. Lines are weak to moderately strong (Wk 150 m8). Surface gravity ( log g) was obtained with the condition that the Fe i and Fe ii lines give the same abundance. The microturbulent velocity (t) was determined by requiring that the Fe i and Ni i lines g ...
The reaction between NH3+ and CH3COOH: a possible process for
... Other authors (Bernstein et al. 2002) have reported a laboratory demonstration that amino acids can be naturally formed from ultraviolet photolysis of icy interstellar grains containing small amounts of materials such as methanol, ammonia, and hydrogen cyanide. The study suggests that at least some ...
... Other authors (Bernstein et al. 2002) have reported a laboratory demonstration that amino acids can be naturally formed from ultraviolet photolysis of icy interstellar grains containing small amounts of materials such as methanol, ammonia, and hydrogen cyanide. The study suggests that at least some ...
the rutherford - santilli neutron
... On environmental grounds, the neutron is one of the largest reservoirs of energy available to mankind because it decays into the proton, a highly energetic electron with the energy of at least 0.78 MeV (that can be easily captured via a metal shield) and the anti-neutrino (that is innocuous, assumin ...
... On environmental grounds, the neutron is one of the largest reservoirs of energy available to mankind because it decays into the proton, a highly energetic electron with the energy of at least 0.78 MeV (that can be easily captured via a metal shield) and the anti-neutrino (that is innocuous, assumin ...
- Mineralogical Society of America
... The advent of multi-collector inductively coupled plasma mass spectrometers (MC-ICPMS), as well as improvements to thermal ionization mass spectrometers (TIMS) in the 1990s has enabled very high precision measurement of isotope ratios for a variety of elements. These mass spectrometers can efficient ...
... The advent of multi-collector inductively coupled plasma mass spectrometers (MC-ICPMS), as well as improvements to thermal ionization mass spectrometers (TIMS) in the 1990s has enabled very high precision measurement of isotope ratios for a variety of elements. These mass spectrometers can efficient ...
Cluster formation in molecular clouds – I. Stellar populations, star
... Gazol & Scalo 2000). The largest areas of star formation occur at the junction of two or more filaments (Schneider et al. 2012). Growing clusters are fed by flow along the filaments (Kirk et al. 2013) which could prolong star formation since radiation and momentum feedback can be released into the l ...
... Gazol & Scalo 2000). The largest areas of star formation occur at the junction of two or more filaments (Schneider et al. 2012). Growing clusters are fed by flow along the filaments (Kirk et al. 2013) which could prolong star formation since radiation and momentum feedback can be released into the l ...
azu_etd_13224_sip1_m
... structure, and host star abundances play in the different stages of planet formation? In this thesis, beginning with a brief literature review in Chapter 2, I trace oxygen and carbon species through these stages to inform how, when, and where planets form. In Chapter 3 I describe a study of the mole ...
... structure, and host star abundances play in the different stages of planet formation? In this thesis, beginning with a brief literature review in Chapter 2, I trace oxygen and carbon species through these stages to inform how, when, and where planets form. In Chapter 3 I describe a study of the mole ...
First axion bounds from a pulsating helium
... white dwarfs (WDs), which are among the most studied classes of stars. These stars represent the final stage of the evolution of low and intermediate mass stars (see [10] and references therein). Our knowledge of the physical processes governing the evolution of WDs relies on solid grounds, since th ...
... white dwarfs (WDs), which are among the most studied classes of stars. These stars represent the final stage of the evolution of low and intermediate mass stars (see [10] and references therein). Our knowledge of the physical processes governing the evolution of WDs relies on solid grounds, since th ...
Here - NASA/IPAC Extragalactic Database
... H ii regions are ionized clouds of gas associated with zones of recent star formation. They are powered by one, a few, or a cluster of massive stars (depending on the resolution at which one is working). The effective temperatures T? of the ionizing stars lie in the range 35 000 – 50 000 K. The nebu ...
... H ii regions are ionized clouds of gas associated with zones of recent star formation. They are powered by one, a few, or a cluster of massive stars (depending on the resolution at which one is working). The effective temperatures T? of the ionizing stars lie in the range 35 000 – 50 000 K. The nebu ...
Elliptical galaxies
... ellipticals are assumed to have formed at high redshift as a result of a rapid collapse of a gas cloud. This gas is rapidly converted into stars by means of a very strong burst Galactic wind powered by the energy injected into the ISM by SNe and stellar winds. carries out the residual gas from the g ...
... ellipticals are assumed to have formed at high redshift as a result of a rapid collapse of a gas cloud. This gas is rapidly converted into stars by means of a very strong burst Galactic wind powered by the energy injected into the ISM by SNe and stellar winds. carries out the residual gas from the g ...
REVIEW Numerical Star-Formation Studies— A Status Report
... of molecular hydrogen gas. Star formation in these clouds is governed by the complex interplay between the gravitational attraction in the gas and agents such as turbulence, magnetic fields, radiation and thermal pressure that resist compression. The competition between these processes determines bot ...
... of molecular hydrogen gas. Star formation in these clouds is governed by the complex interplay between the gravitational attraction in the gas and agents such as turbulence, magnetic fields, radiation and thermal pressure that resist compression. The competition between these processes determines bot ...
Annual Report 2014 - Max Planck Institute for Astrophysics
... the directorship of Ludwig Biermann. It was estab- MPA has had an internationally-recognized numerlished as an offshoot of the Max-Planck-Institut für ical astrophysics program that was long unparalPhysik, which at that time had just moved from leled by any other institution of similar size. Göttinge ...
... the directorship of Ludwig Biermann. It was estab- MPA has had an internationally-recognized numerlished as an offshoot of the Max-Planck-Institut für ical astrophysics program that was long unparalPhysik, which at that time had just moved from leled by any other institution of similar size. Göttinge ...
The First Galaxies: Assembly under Radiative Feedback from the
... heats the gas inside the first halos and the intergalactic medium (IGM). The associated increase in pressure drives the gas outside halos with virial temperatures . 104 K, suppressing star formation in both minihalos and the first atomic cooling halos (e.g., Thoul & Weinberg 1996; Barkana & Loeb 199 ...
... heats the gas inside the first halos and the intergalactic medium (IGM). The associated increase in pressure drives the gas outside halos with virial temperatures . 104 K, suppressing star formation in both minihalos and the first atomic cooling halos (e.g., Thoul & Weinberg 1996; Barkana & Loeb 199 ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.